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• W4210286588 abstract "Tidal heating is often used to interpret radius anomaly of hot Jupiters (i.e. radii of a large fraction of hot Jupiters are in excess of 1.2 Jupiter radius which cannot be interpreted by the standard theory of planetary evolution). In this paper we find that tidal heating induces another phenomenon runaway inflation (i.e. planet inflation becomes unstable and out of control when tidal heating rate is above its critical value). With sufficiently strong tidal heating, luminosity initially increases with inflation, but across its peak it decreases with inflation such that heating is stronger than cooling and runaway inflation occurs. In this mechanism, the opacity near radiative-convective boundary (RCB) scales approximately as temperature to the fourth power and heat cannot efficiently radiate away from planet interior, which induces runaway inflation (similar to a tight lid on a boiling pot). Based on this mechanism, we find that radii of hot Jupiters cannot exceed $2.2R_J$, which is in good agreement with the observations. We also give an upper limit for orbital eccentricity of hot Jupiters. Moreover, by comparison to the observations we infer that tidal heating locates near RCB." @default.
• W4210286588 created "2022-02-08" @default.
• W4210286588 creator A5005505236 @default.
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• W4210286588 date "2022-01-31" @default.
• W4210286588 modified "2023-10-16" @default.
• W4210286588 title "Why hot Jupiters can be large but not too large" @default.
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• W4210286588 doi "https://doi.org/10.1093/mnras/stac169" @default.
• W4210286588 hasPublicationYear "2022" @default.
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